The Simulated HI Sky at low redshift

TL;DR

This paper uses cosmological hydrodynamic simulations to study the distribution and emission properties of neutral hydrogen in the low-redshift universe, especially below the typical detection threshold, and compares results with observations.

Contribution

It provides a detailed simulation-based analysis of HI distribution below NHI ~ 10^19 cm-2, including self-shielding and molecular hydrogen effects, matching observational data.

Findings

Simulated HI distribution matches observed column density range from 10^14 to 10^21 cm-2.

The simulation accurately reproduces the HI mass function and two-point correlation function.

Simulated maps can predict observations for current and future telescopes.

Abstract

Observations of intergalactic neutral hydrogen can provide a wealth of information about structure and galaxy formation, potentially tracing accretion and feedback processes on Mpc scales. Below a column density of NHI ~ 10^19 cm-2, the "edge" or typical observational limit for HI emission from galaxies, simulations predict a cosmic web of extended emission and filamentary structures. We study the distribution of neutral hydrogen and its 21cm emission properties in a cosmological hydrodynamic simulation, to gain more insights into the distribution of HI below NHI ~ 10^19 cm-2. Such Lyman Limit systems are expected to trace out the cosmic web, and are relatively unexplored. Beginning with a 32 h^-1 Mpc simulation, we extract the neutral hydrogen component by determining the neutral fraction, including a post-processed correction for self-shielding based on the thermal pressure. We take into account molecular hydrogen, assuming an average density ratio Omega_H2 / Omega_HI = 0.3 at z = 0. The statistical properties of the HI emission are compared with observations, to assess the reliability of the simulation. The simulated HI distribution robustly describes the full column density range between NHI ~ 10^14 and NHI ~ 10^21 cm-2 and agrees very well with available measurements from observations. Furthermore there is good correspondence in the statistics when looking at the two-point correlation function and the HI mass function. The reconstructed maps are used to simulate observations of existing and future telescopes by adding noise and taking account of the sensitivity of the telescopes. The general agreement in statistical properties of HI suggests that neutral hydrogen as modeled in this hydrodynamic simulation is a fair representation of that in the Universe. (abridged)